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arxiv: 2606.25794 · v1 · pith:DQZFBWCAnew · submitted 2026-06-24 · 🌌 astro-ph.EP · astro-ph.IM

Substructures in Planet-Forming Disks with the SKAO

Yinhao Wu , Jessica Speedie , Sebasti\'an P\'erez , John D. Ilee , Takahiro Ueda , Claudia Toci , Daniel J. Price , Asmita Bhandare
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Eleonora Bianchi Tilman Birnstiel Richard A. Booth Tyler L. Bourke Gemma Busquet Simon Casassus Yi-Xian Chen Claudio Codella Nicol\'as Cuello Ruobing Dong Antonio Garufi Greta Guidi Cassandra Hall Haochang Jiang Izaskun Jim\'enez-Serra Hauyu Baobab Liu Mayank Narang Elenia Pacetti Jaime Pineda Paola Pinilla Linda Podio Danai Polychroni Giovanni Sabatini Eugenio Schisano Leonardo Testi Diego Turrini Marion Villenave David Wilner
This is my paper

Pith reviewed 2026-06-25 19:33 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IM
keywords protoplanetary disksdisk substructuresSKA-Midplanet formationdust thermal emissionradio continuumgaps and rings
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The pith

SKA-Mid Band 5b continuum observations at 12.5 GHz will resolve protoplanetary disk substructures to constrain their origins and planet-assembly roles via dust thermal emission.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper reviews persistent unknowns about substructures such as rings, gaps, spirals, and asymmetries in gas and dust disks around young stars, which serve as sites of planet formation. It argues that SKA-Mid's high-resolution radio continuum data at centimeter wavelengths can supply fresh constraints by imaging the same features through dust thermal emission at longer wavelengths than typical millimeter studies. A sympathetic reader would care because these substructures likely shape how planets grow and migrate, and resolving their true properties could link disk morphology to the observed diversity of exoplanets. The chapter focuses on specific open questions in origin, role, and physical characteristics that the new resolution and wavelength coverage can target.

Core claim

SKA-Mid Band 5b continuum observations, offering angular resolutions of ~0.05'' (~0.15'') with AA4 (AA*) at 12.5 GHz / 2.4 cm, will enable new progress on the origin of disk substructures, their role in planet assembly, and their true properties, with a lens on dust thermal emission.

What carries the argument

SKA-Mid Band 5b continuum observations at 12.5 GHz with ~0.05 arcsecond resolution, which image dust thermal emission to compare substructures across wavelengths.

If this is right

  • Substructures resolved at 2.4 cm can be compared to millimeter-wave maps to test whether they trace identical physical features or different dust populations.
  • Thermal emission data at this frequency will constrain grain sizes and optical depths inside rings and gaps, narrowing possible formation mechanisms.
  • Spatial distributions of substructures measured at high resolution will clarify whether they promote or suppress planetesimal growth.
  • Multi-epoch or multi-configuration SKA data can track time evolution of asymmetries and vortices linked to planet-disk interactions.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the wavelength comparison works, joint SKA-ALMA campaigns could become standard for mapping full dust size distributions across entire disks.
  • Non-detections at centimeter wavelengths for some millimeter substructures would imply strong radial drift or grain growth that current models underpredict.
  • The technique might extend to fainter or more distant disks once sensitivity improves, testing whether substructure statistics vary with stellar mass or environment.

Load-bearing premise

The assumption that continuum observations at 12.5 GHz will detect and characterize the same substructures seen at shorter wavelengths in a manner that directly constrains their physical origin and planet-formation role.

What would settle it

SKA-Mid observations at 12.5 GHz that either detect no substructures where shorter-wavelength data show clear ones, or yield structures whose properties show no systematic link to planet-formation indicators such as gap widths or dust trapping.

Figures

Figures reproduced from arXiv: 2606.25794 by Antonio Garufi, Asmita Bhandare, Cassandra Hall, Claudia Toci, Claudio Codella, Danai Polychroni, Daniel J. Price, David Wilner, Diego Turrini, Elenia Pacetti, Eleonora Bianchi, Eugenio Schisano, Gemma Busquet, Giovanni Sabatini, Greta Guidi, Haochang Jiang, Hauyu Baobab Liu, Izaskun Jim\'enez-Serra, Jaime Pineda, Jessica Speedie, John D. Ilee, Leonardo Testi, Linda Podio, Marion Villenave, Mayank Narang, Nicol\'as Cuello, Paola Pinilla, Richard A. Booth, Ruobing Dong, Sebasti\'an P\'erez, Simon Casassus, Takahiro Ueda, Tilman Birnstiel, Tyler L. Bourke, Yinhao Wu, Yi-Xian Chen.

Figure 1
Figure 1. Figure 1: Schematic illustrations of the dust substructures observed in protoplanetary disks in mm continuum emission. The substructures are qualitatively organized in order of increasing asymmetry (to the right), and increasing extent of central emission (going downward). Within each disk illustration, yellow colour highlights the substructure that is labelled at the top of each column. Each illustration is based o… view at source ↗
Figure 2
Figure 2. Figure 2: An overview of continuum observations, obtained in the last decade, spatially resolving the distribution of dust in the disk around HL Tau at (sub-)mm wavelengths. SKA-Mid will extend our view to sub-cm wavelengths that are presently unexplored, providing sensitivity to larger grains and optically thinner emission. This chapter focuses on continuum observations with Band 5b (8.3 − 15.4 GHz observing freque… view at source ↗
Figure 3
Figure 3. Figure 3: Maximum dust sizes regulated by radial drift (yellow solid line) and collisional fragmentation (green solid lines) in protoplanetary disks (Birnstiel, 2024), overlaid with the typical dust sizes probed by ALMA, VLA, and SKA. The maximum sizes for drift and fragmentation are computed assuming a turbulence strength of 𝛼 = 3× 10−4 and a gas surface density profile of Σg = 1000 (𝑟/au) −1 exp(−𝑟/50 au) g cm−2 w… view at source ↗
Figure 4
Figure 4. Figure 4: Predicted radial intensity profiles of the HL Tau disk at 12.5 GHz (SKA-Mid Band 5b) with AA* (left panel) and AA4 (right panel). In each panel, the underlying model profile in 𝜇Jy arcsec−2 is scaled and spatially convolved to 𝜇Jy beam−1 , where the beam is a Gaussian fit to the PSF cross section that is shown in the top right corner. The PSFs are generated from 𝑢𝑣-coverage simulations, and weighted with a… view at source ↗
Figure 5
Figure 5. Figure 5: HL Tau through the eyes of SKA-Mid: Predicted continuum images of the HL Tau disk at 12.5 GHz (Band 5b) with AA* (middle panel) and AA4 (rightmost panel). The synthesized beams shown in the bottom left corners are generated from 𝑢𝑣-coverage simulations, and weighted with a Briggs robust parameter of −1. Dish SKA008 is excluded from AA*. The achieved sensitivity is 0.115 𝜇Jy beam−1 and 0.049 𝜇Jy beam−1 by A… view at source ↗
Figure 6
Figure 6. Figure 6: Simulated SKA Mid AA4 12.5 GHz observations of six protoplanetary disks with improving angular resolution (0.5 ′′ , 0.25′′ , 0.12′′ and 0.08′′) and increasing integration time (30, 100, 300 and 1000 hrs). Each panel is peak normalised and shown with a power law stretch. 18 [PITH_FULL_IMAGE:figures/full_fig_p018_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of array layout, simulated 𝑢𝑣 coverage, and PSF cross sections between array assemblies: AA* (left panels), AA* including dish SKA008 (middle panels) and AA4 (right panels). The 𝑢𝑣-coverage simulations are performed with the SKAO Observing Support Tool ska_ost_array_config python package. The pointing phase center is taken to be the celestial south pole (−90.0 ◦ declination), such that, after th… view at source ↗
read the original abstract

Disks of gas and dust orbiting young stars are the arenas and material reservoirs for planet formation. Over the past decade, multiwavelength observations, from infrared to radio, have resolved the spatial distribution of hundreds of protoplanetary disks in nearby star-forming regions, revealing a diverse zoo of substructures. These substructures are morphological features such as rings, gaps, spirals, vortices, asymmetries, warps, or clumps that trace variations in density, temperature, or composition relative to an otherwise smooth distribution of gas and dust. Many unknowns persist as to the origin of these substructures, their role in planet assembly, and their true properties. SKA-Mid Band 5b continuum observations, offering angular resolutions of $\sim 0.05''$ ($\sim 0.15''$) with AA4 (AA*) at $12.5$ GHz / $2.4$ cm, will enable new progress at this frontier. In this chapter, we outline the open questions in the field of disk substructure that SKA-Mid is uniquely poised to address, with a lens on dust thermal emission.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 0 minor

Summary. The manuscript is a perspective chapter outlining open questions on the origins of substructures (rings, gaps, spirals, etc.) in protoplanetary disks, their role in planet assembly, and their physical properties. It argues that SKA-Mid Band 5b continuum observations at 12.5 GHz / 2.4 cm, achieving angular resolutions of ~0.05'' (AA4) or ~0.15'' (AA*), will enable new progress on these questions specifically through dust thermal emission.

Significance. If the technical assumptions hold, the paper provides a useful forward-looking roadmap for how SKA-Mid can complement existing mm-wave facilities like ALMA by accessing cm-wavelength regimes, potentially constraining grain properties and substructure origins in a manner not currently accessible.

major comments (1)
  1. [Abstract] Abstract (paragraph on open questions): The claim that Band 5b observations 'will enable new progress' on substructure origins and planet-assembly role via dust thermal emission is load-bearing but rests on the unexamined assumption that 12.5 GHz morphology directly maps to the same density/temperature variations seen at 1.3 mm. The text supplies no quantitative estimate of how substructure contrast or location would change under grain-size-dependent opacity (κ_ν ∝ ν^β(a_max)), size-dependent radial drift, or trapping, nor does it address possible free-free contamination or optical-depth shifts that could alter the inferred physical origin.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive report and for identifying a key point about the assumptions underlying our forward-looking claims. We address the major comment below in detail. As this is a perspective chapter focused on open questions rather than new modeling, we will incorporate clarifications to strengthen the presentation without altering the core message.

read point-by-point responses

  1. Referee: [Abstract] Abstract (paragraph on open questions): The claim that Band 5b observations 'will enable new progress' on substructure origins and planet-assembly role via dust thermal emission is load-bearing but rests on the unexamined assumption that 12.5 GHz morphology directly maps to the same density/temperature variations seen at 1.3 mm. The text supplies no quantitative estimate of how substructure contrast or location would change under grain-size-dependent opacity (κ_ν ∝ ν^β(a_max)), size-dependent radial drift, or trapping, nor does it address possible free-free contamination or optical-depth shifts that could alter the inferred physical origin.

    Authors: We agree that the abstract is necessarily concise and that the claim would benefit from explicit acknowledgment of wavelength-dependent effects. As a perspective piece, the manuscript does not perform or cite new quantitative radiative-transfer calculations comparing 1.3 mm and 12.5 GHz morphologies; instead it highlights that cm-wave data will access a different grain-size regime and optical-depth regime, thereby providing independent constraints on the very mechanisms (trapping, drift, opacity variations) the referee mentions. The body of the text already notes that longer wavelengths preferentially trace larger grains and can help discriminate between substructure origins, but we concede that a short, qualitative discussion of possible contrast changes, free-free contributions, and optical-depth shifts is absent. We will therefore revise the abstract to qualify the claim and add one paragraph (likely in the introduction or a new short subsection) that outlines these caveats while emphasizing that SKA-Mid observations themselves will supply the multi-wavelength data needed to test them. This constitutes a targeted clarification rather than a change in scientific content. revision: yes

Circularity Check

0 steps flagged

No circularity: qualitative forward-looking discussion with no derivations or equations

full rationale

The paper is a perspective chapter outlining open questions in disk substructures and how SKA-Mid Band 5b observations may address them. It contains no equations, derivations, fitted parameters, predictions of quantitative results, or load-bearing self-citations that reduce to inputs by construction. The central claim is a qualitative statement about observational capability enabling progress, with no reduction of any result to a fitted input or self-referential definition. This matches the default expectation of no significant circularity for papers without mathematical chains.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The paper relies on established domain knowledge of protoplanetary disk substructures from prior infrared and radio observations plus standard SKA instrument parameters; no new free parameters, ad-hoc axioms, or invented entities are introduced.

axioms (1)
  • domain assumption Standard assumptions about the detectability and interpretability of dust thermal emission at centimeter wavelengths in protoplanetary disks.
    Invoked when arguing that SKA-Mid Band 5b observations will address open questions about substructure properties.

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Reference graph

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